Conference on the theory of atoms and molecules

Sokolov, N. D.

doi:10.1007/bf01128435

Cited by 26 publications

(29 citation statements)

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“…Letelier showed that combinations between perfect and null fluids can give rise to anisotropic fluids [36]. Other reasons can be taken into account to generate anisotropies like pion condensation [37], strong electromagnetic field [38] and phase transition [39].…”

Section: Introductionmentioning

confidence: 99%

Stable and self-consistent compact star models in teleparallel gravity

Nashed

Capozziello

2020

Eur. Phys. J. C

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In the framework of Teleparallel Gravity, we derive a charged non-vacuum solution for a physically symmetric tetrad field with two unknown functions of radial coordinate. The field equations result in a closed-form adopting particular metric potentials and a suitable anisotropy function combined with the charge. Under these circumstances, it is possible to obtain a set of configurations compatible with observed pulsars. Specifically, boundary conditions for the interior spacetime are applied to the exterior Reissner–Nordström metric to constrain the radial pressure that has to vanish through the boundary. Starting from these considerations, we are able to fix the model parameters. The pulsar $$\textit{PSR J 1614-2230}$$ PSR J 1614 - 2230 , with estimated mass $$M= 1.97 \pm 0.04\, M_{\circledcirc },$$ M = 1.97 ± 0.04 M ⊚ , and radius $$R= 9.69 \pm 0.2$$ R = 9.69 ± 0.2 km is used to test numerically the model. The stability is studied, through the causality conditions and adiabatic index, adopting the Tolman–Oppenheimer–Volkov equation. The mass–radius (M, R) relation is derived. Furthermore, the compatibility of the model with other observed pulsars is also studied. We reasonably conclude that the model can represent realistic compact objects.

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Section: Introductionmentioning

confidence: 99%

Stable and self-consistent compact star models in teleparallel gravity

Nashed

Capozziello

2020

Eur. Phys. J. C

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“…Some argument against the existence of anisotropy could be verifiable through the existence of a solid core or the presence of a type 3A fluid; see the work of Kippenhahn and Weigert [6]. On the other hand, this can arise from different kinds of phase transition and pion condensation as pointed out by Sokolov and Sawyer [7]. The structure of compact objects in general relativity will depend on several parameters, including fluid and magnetic stresses, entropy gradients, composition, heat flow and neutrino emission.…”

Section: Introductionmentioning

confidence: 99%

A new model for spherically symmetric anisotropic compact star

Gupta²,

et al. 2016

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In this article we obtain a new anisotropic solution for Einstein's field equations of embedding class one metric. The solution represents realistic objects such as Her X-1 and RXJ 1856-37. We perform a detailed investigation of both objects by solving numerically the Einstein field equations with anisotropic pressure. The physical features of the parameters depend on the anisotropic factor i.e. if the anisotropy is zero everywhere inside the star then the density and pressures will become zero and the metric turns out to be flat. We report our results and compare with the above mentioned two compact objects as regards a number of key aspects: the central density, the surface density onset and the critical scaling behaviour, the effective mass and radius ratio, the anisotropization with isotropic initial conditions, adiabatic index and red shift. Along with this we have also made a comparison between the classical limit and theoretical model treatment of the compact objects. Finally we discuss the implications of our findings for the stability condition in a relativistic compact star.

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“…Bowers and Liang [23] did pioneer work in describing possible significance of locally anisotropic pressure distribution in relativistic spherical matter configurations and found that anisotropy may have worthwhile effects on parameters controlling the hydrostatic equilibrium of celestial systems. The anisotropy within stellar systems can be observed through number of interested interconnected mechanisms, e.g., existence of strong electric and magnetic interactions [24], condensations of pions [25], phase transitions [26], the presence of vacuum core [27], even the emergence of gravitational waves from non-static meridional axial stellar structures [28] etc. It can be demonstrated that the mixture of two fluid configurations can be mathematically treated as an anisotropic framework.…”

Section: Introductionmentioning

confidence: 99%

Influence of modification of gravity on the dynamics of radiating spherical fluids

Yousaf¹,

Bamba²,

Bhatti³

2016

Phys. Rev. D

188

125

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We explore the evolutionary behaviors of compact objects in a modified gravitational theory with the help of structure scalars. Particularly, we consider the spherical geometry coupled with heat and radiation emitting shearing viscous matter configurations. We construct structure scalars by splitting the Riemann tensor orthogonally in f (R, T ) gravity with and without constant R and T constraints, where R is the Ricci scalar and T is the trace of the energy-momentum tensor. We investigate the influence of modification of gravity on the physical meaning of scalar functions for radiating spherical matter configurations. It is explicitly demonstrated that even in modified gravity, the evolutionary phases of relativistic stellar systems can be analyzed through the set of modified scalar functions.

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Conference on the theory of atoms and molecules

Cited by 26 publications

References 0 publications

Stable and self-consistent compact star models in teleparallel gravity

Stable and self-consistent compact star models in teleparallel gravity

A new model for spherically symmetric anisotropic compact star

Influence of modification of gravity on the dynamics of radiating spherical fluids

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